Crab Pulsar

Crab Pulsar

The Crab Nebula, which contains the Crab Pulsar. Image combines optical data from Hubble (in red) and X-ray images from Chandra (in blue). NASA/CXC/ASU/J. Hester et al.[1]
Observation data Epoch J2000      Equinox J2000
Constellation	Taurus
Right ascension	05h 34m 31.97s
Declination	+22° 00' 52.1"
Apparent magnitude (V)	16.5
Characteristics
Evolutionary stage	Neutron star
U−B color index	-0.45
B−V color index	+0.5
Astrometry
Proper motion (μ)	RA: -14.7±0.8[2] mas/yr Dec.: 2.0±0.8[2] mas/yr
Distance	2200[2] pc
Details
Mass	1.4[3] M☉
Radius	~6995143781500000000♠1.437815×10−5[3] R☉
Luminosity	? L☉
Temperature	Center (modeled): ~7008300000000000000♠3×108[3] K Surface: ~1.6 × 106 K
Rotation	33.5028583 ms[2]
Age	963 years
Other designations
SNR G184.6-05.8, 2C 481, 3C 144.0, SN 1054A, 4C 21.19, NGC 1952, PKS 0531+219, PSR B0531+21, PSR J0534+2200, CM Tau.
Database references
SIMBAD	pulsar data

The Crab Pulsar (PSR B0531+21) is a relatively young neutron star. The star is the central star in the Crab Nebula, a remnant of the supernova SN 1054, which was widely observed on Earth in the year 1054.^[4][5][6] Discovered in 1968, the pulsar was the first to be connected with a supernova remnant.^[7]

The Crab Pulsar is one of very few pulsars to be identified optically. The optical pulsar is roughly 20 kilometres (12 mi) in diameter and the pulsar "beams" rotate once every 33 milliseconds, or 30 times each second.^[3] The outflowing relativistic wind from the neutron star generates synchrotron emission, which produces the bulk of the emission from the nebula, seen from radio waves through to gamma rays. The most dynamic feature in the inner part of the nebula is the point where the pulsar's equatorial wind slams into the surrounding nebula, forming a termination shock. The shape and position of this feature shifts rapidly, with the equatorial wind appearing as a series of wisp-like features that steepen, brighten, then fade as they move away from the pulsar into the main body of the nebula. The period of the pulsar's rotation is slowing by 38 nanoseconds per day due to the large amounts of energy carried away in the pulsar wind.^[8]

The Crab Nebula is often used as a calibration source in X-ray astronomy. It is very bright in X-rays and the flux density and spectrum are known to be constant, with the exception of the pulsar itself. The pulsar provides a strong periodic signal that is used to check the timing of the X-ray detectors. In X-ray astronomy, 'crab' and 'millicrab' are sometimes used as units of flux density. A millicrab corresponds to a flux density of about 6989240000000000000♠2.4×10⁻¹¹ erg s⁻¹ cm⁻² (6986239999999999999♠2.4×10⁻¹⁴ W m⁻²) in the 2–10 keV X-ray band, for a "crab-like" X-ray spectrum, which is roughly a powerlaw in photon energy, I = 9.5 E^−1.1. Very few X-ray sources ever exceed one crab in brightness.

History of observation

X-ray picture of Crab pulsar, taken by Chandra.

The Crab Nebula was identified as the remnant of SN 1054 by 1939. Astronomers then searched for the nebula's central star. There were two candidates, referred to in the literature as the "north following" and "south preceding" stars. In September 1942, Walter Baade ruled out the "north following" star, but found the evidence inconclusive for the "south preceding" star.^[9] Rudolf Minkowski, in the same issue of The Astrophysical Journal as Baade, advanced spectral arguments claiming that the "evidence admits, but does not prove, the conclusion that the south preceding star is the central star of the nebula".^[10]

In late 1968, David H. Staelin and Edward C. Reifenstein III reported the discovery of two pulsating radio sources "near the crab nebula that could be coincident with it" using the 300-foot Green Bank radio antenna.^[11] They were given the designations NP 0527 and NP 0532. The period and location of the Crab Nebula pulsar NP 0532 was discovered by Richard Lovelace and collaborators November 10, 1968 at the Arecibo radio observatory.^[12]

A slow-motion animation of the Crab Pulsar taken at 800 nm wavelength (near-infrared) using a Lucky Imaging camera from Cambridge University, showing the bright pulse and fainter interpulse.

A subsequent study by them including William D. Brundage also found that the NP 0532 source is located at the Crab Nebula.^[13] A radio source was also reported coincident with the crab nebula in late 1968 by L. I. Matveenko in Soviet Astronomy.^[14]

Optical pulsations were first reported by Cocke, Disney, and Taylor using the 36-inch telescope on Kitt Peak of the Steward Observatory of the University of Arizona.^[15] Their discovery was confirmed by Nather, Warner, and Macfarlane.^[16]

Jocelyn Bell Burnell, who co-discovered the first pulsar PSR B1919+21 in 1967, relates that in the late 1950s a woman viewed the Crab Nebula source at the University of Chicago's telescope, then open to the public, and noted that it appeared to be flashing. The astronomer she spoke to, Elliot Moore, disregarded the effect as scintillation, despite the woman's protestation that as a qualified pilot she understood scintillation and this was something else. Bell Burnell notes that the 30 Hz frequency of the Crab Nebula optical pulsar is difficult for many people to see.^[17][18]

The Crab Pulsar was the first pulsar for which the spin-down limit was broken using several months of data of the LIGO observatory. Most pulsars do not rotate at constant rotation frequency, but can be observed to slow down at a very slow rate (3.7e-10 Hz/s in case of the Crab). This spin-down can be explained as a loss of rotation energy due to various mechanisms. The spin-down limit is a theoretical upper limit of the amplitude of gravitational waves that a pulsar can emit, assuming that all the losses in energy are converted to gravitational waves. No gravitational waves being observed at the expected amplitude and frequency (after correcting for the expected Doppler shift) is therefore a proof that other mechanisms must be responsible for the loss in energy. The non-observation so far is not totally unexpected, since physical models of the rotational symmetry of pulsars puts a more realistic upper limit on the amplitude of gravitational waves several orders of magnitude below the spin-down limit. It is hoped that with the improvement of the sensitivity of gravitational wave instruments and the use of longer stretches of data, gravitational waves emitted by pulsars will be observed in future.^[19] The only other pulsar for which the spin-down limit was broken so far is the Vela Pulsar.

References

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